I'm currently a Postdoctoral research associate at the Department of Astrophysical Sciences at Princeton University. My research interests include High Performance Computing, Parallel and GPU computing, Computational Fluid Dynamics and Planet formation, with emphasis in planet-disc interaction.
In this work, we have presented a novel implementation of an arbitrarily high-order SD method, with a second order FV solver as fallback scheme. We have demonstrated that the resulting method has robust shock-capturing capabilities.
We have adapted our nested-meshes version of the fargo3d code to perform simulations of a freely evolving, luminous planet in a thermally diffusive gaseous disc around a solar-mass star. The implementation allowed us to improve the resolution of previous work (Eklund & Masset 2017), and to get converged results for the eccentricity reached at larger time, or asymptotic eccentricity, by a low-mass planet as a function of its luminosity.
We have performed high-resolution simulations in the subsonic regime in two and three dimensions that resolve the Bondi radius of a perturber travelling at constant speed in a gas with initially uniform density and temperature. We have found that for perturbers with sufficiently small mass, the net force is in agreement with that obtained from linear theory (Masset & Velasco-Romero 2017). At larger masses, the thermal forces are smaller than those given by linear theory.
We have conducted extensive numerical simulations in order to check the impact of thermal effects on the dynamical friction on to a massive perturber, both with and without intrinsic luminosity (i.e. with or without radiative feedback). Owing to the wide interval of length scales required to capture accurately thermal effects, we had to resort to nested meshes, that we implemented in the GPU version of the FARGO3D code.
